Insights into the emission of the blazar 1ES 1011+496 through unprecedented broadband observations during 2011 and 2012
Insights into the emission of the blazar 1ES 1011+496 through unprecedented broadband observations during 2011 and 2012
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DOI：
10.1051/0004-6361/201527176
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发表时间：
2016-03
影响因子：
6.5
通讯作者：
J. Aleksic;S. Ansoldi;L. Antonelli;P. Antoranz;C. Arcaro;A. Babić;P. Bangale;U. D. Almeida;J. Barrio;J. Gonz'alez;W. Bednarek;E. Bernardini;B. Biasuzzi;A. Biland;O. Blanch;S. Bonnefoy;G. Bonnoli;F. Borracci;T. Bretz;E. Carmona;A. Carosi;P. Colin;E. Colombo;J. Contreras;J. Cortina;S. Covino;P. D. Vela;F. Dazzi;A. Angelis;G. Caneva;B. Lotto;E. Wilhelmi;C. Mendez;F. D. Pierro;D. D. Prester-D.;D. Dorner;M. Doro;S. Einecke;D. Eisenacher;D. Elsaesser;A. Fern'andez-Barral;D. Fidalgo;M. Fonseca;L. Font;K. Frantzen;C. Fruck;D. Galindo;R. L'opez;M. Garczarczyk;D. G. Terrats;M. Gaug;N. Godinovic;A. G. Muñoz;S. Gozzini;D. Hadasch;Y. Hanabata;M. Hayashida;J. Herrera;J. Hose;D. Hrupec;W. Idec;V. Kadenius;H. Kellermann;M. Knoetig;K. Kodani;Y. Konno;J. Krause;H. Kubo;J. Kushida;A. Barbera;D. Lelas;N. Lewandowska;E. Lindfors;S. Lombardi;F. Longo;M. L'opez;R. López-Coto;A. L'opez-Oramas;E. Lorenz;I. Lozano;M. Makariev;K. Mallot;G. Maneva;K. Mannheim;L. Maraschi;B. Marcote;M. Mariotti;M. Mart'inez;D. Mazin;U. Menzel;J. Miranda;R. Mirzoyan;A. Moralejo;P. Munar-Adrover;D. Nakajima;V. Neustroev;A. Niedźwiecki;M. N. Rosillo;K. Nilsson;K. Nishijima;K. Noda;R. Orito;A. Overkemping;S. Paiano;M. Palatiello;D. Paneque;R. Paoletti;J. Paredes;X. Paredes-Fortuny;M. Persic;J. Poutanen;P. Moroni;E. Prandini;I. Puljak;R. Reinthal;W. Rhode;M. Ribó;J. Rico;J. Garcia;T. Saito;K. Saito;K. Satalecka;V. Scalzotto;V. Scapin;T. Schweizer;S. Shore;A. Sillanpää;J. Sitarek;I. Šnidarić;D. Sobczynska;A. Stamerra;T. Steinbring;M. Strzys;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzić;D. Tescaro;M. Teshima;J. Thaele;D. Torres;T. Toyama;A. Treves;P. Vogler;M. Will;R. Zanin;S. Buson;F. D’Ammando;A. Lähteenmäki;T. Hovatta;Y. Kovalev;M. Lister;W. Max-Moerbeck;C. Mundell;A. Pushkarev;E. Rastorgueva-Foi;A. Readhead;J. Richards;J. Tammi;D. Sanchez;M. Tornikoski;T. Savolainen;I. Steele
中科院分区：
文献类型：
--
作者：
J. Aleksic;S. Ansoldi;L. Antonelli;P. Antoranz;C. Arcaro;A. Babić;P. Bangale;U. D. Almeida;J. Barrio;J. Gonz'alez;W. Bednarek;E. Bernardini;B. Biasuzzi;A. Biland;O. Blanch;S. Bonnefoy;G. Bonnoli;F. Borracci;T. Bretz;E. Carmona;A. Carosi;P. Colin;E. Colombo;J. Contreras;J. Cortina;S. Covino;P. D. Vela;F. Dazzi;A. Angelis;G. Caneva;B. Lotto;E. Wilhelmi;C. Mendez;F. D. Pierro;D. D. Prester-D.;D. Dorner;M. Doro;S. Einecke;D. Eisenacher;D. Elsaesser;A. Fern'andez-Barral;D. Fidalgo;M. Fonseca;L. Font;K. Frantzen;C. Fruck;D. Galindo;R. L'opez;M. Garczarczyk;D. G. Terrats;M. Gaug;N. Godinovic;A. G. Muñoz;S. Gozzini;D. Hadasch;Y. Hanabata;M. Hayashida;J. Herrera;J. Hose;D. Hrupec;W. Idec;V. Kadenius;H. Kellermann;M. Knoetig;K. Kodani;Y. Konno;J. Krause;H. Kubo;J. Kushida;A. Barbera;D. Lelas;N. Lewandowska;E. Lindfors;S. Lombardi;F. Longo;M. L'opez;R. López-Coto;A. L'opez-Oramas;E. Lorenz;I. Lozano;M. Makariev;K. Mallot;G. Maneva;K. Mannheim;L. Maraschi;B. Marcote;M. Mariotti;M. Mart'inez;D. Mazin;U. Menzel;J. Miranda;R. Mirzoyan;A. Moralejo;P. Munar-Adrover;D. Nakajima;V. Neustroev;A. Niedźwiecki;M. N. Rosillo;K. Nilsson;K. Nishijima;K. Noda;R. Orito;A. Overkemping;S. Paiano;M. Palatiello;D. Paneque;R. Paoletti;J. Paredes;X. Paredes-Fortuny;M. Persic;J. Poutanen;P. Moroni;E. Prandini;I. Puljak;R. Reinthal;W. Rhode;M. Ribó;J. Rico;J. Garcia;T. Saito;K. Saito;K. Satalecka;V. Scalzotto;V. Scapin;T. Schweizer;S. Shore;A. Sillanpää;J. Sitarek;I. Šnidarić;D. Sobczynska;A. Stamerra;T. Steinbring;M. Strzys;L. Takalo;H. Takami;F. Tavecchio;P. Temnikov;T. Terzić;D. Tescaro;M. Teshima;J. Thaele;D. Torres;T. Toyama;A. Treves;P. Vogler;M. Will;R. Zanin;S. Buson;F. D’Ammando;A. Lähteenmäki;T. Hovatta;Y. Kovalev;M. Lister;W. Max-Moerbeck;C. Mundell;A. Pushkarev;E. Rastorgueva-Foi;A. Readhead;J. Richards;J. Tammi;D. Sanchez;M. Tornikoski;T. Savolainen;I. Steele
1ES 1011+496 (z=0.212) 是在 2007 年用 MAGIC 在极高能量（VHE，E >100 GeV）γ 射线中发现的。由于缺乏较低能量的同步数据，导致宽带光谱能量分布 (SED) 的表征相当不完整。我们研究了源特性和发射机制，探讨简单的单区同步加速器自康普顿（SSC）场景是否能够解释观测到的宽带光谱。我们分析了 MAGIC、Fermi-LAT、Swift、KVA、OVRO 和 Mets\"ahovi 收集的 2011 年和 2012 年的 VHE 射电数据，以及来自利物浦望远镜和 MOJAVE 的光学偏振数据和射电图。VHE 光谱符合简单的幂律，光子指数为 3.69±0.22，通量高于 150 GeV (1.46±0.16)×10−11 ph cm−2 s−1。1ES 1011+496 在所有观测波长下均处于静止状态，仅显示出从射电到 X 射线的中等变化，在光学中测量到小于 10% 的低偏振度，而在射电射流中观察到一些高达 60% 的明亮特征。射电图显示出 1.8±0.4c 的超光速运动，这是迄今为止在高频峰值 BL Lac 中测量到的最高速度。首次可以完全表征 1ES 1011+496 的宽带 SED 中的高能凹凸，这使得在单区 SSC 场景中能够进行更可靠的解释。光发射起源于一些明亮的射电特征，而光学中的低偏振可能是由于具有不同磁场方向的射电射流部分对光发射的贡献。
1ES 1011+496 (z=0.212) was discovered in very high energy (VHE, E >100 GeV) γ-rays with MAGIC in 2007. The absence of simultaneous data at lower energies led to a rather incomplete characterization of the broadband spectral energy distribution (SED). We study the source properties and the emission mechanisms, probing whether a simple one-zone synchrotron-self-Compton (SSC) scenario is able to explain the observed broadband spectrum. We analyzed VHE to radio data from 2011 and 2012 collected by MAGIC, Fermi-LAT, Swift, KVA, OVRO, and Mets\"ahovi in addition to optical polarimetry data and radio maps from the Liverpool Telescope and MOJAVE. The VHE spectrum was fit with a simple power law with a photon index of 3.69±0.22 and a flux above 150 GeV of (1.46±0.16)×10−11 ph cm−2 s−1. 1ES 1011+496 was found to be in a generally quiescent state at all observed wavelengths, showing only moderate variability from radio to X-rays. A low degree of polarization of less than 10% was measured in optical, while some bright features polarized up to 60% were observed in the radio jet. A similar trend in the rotation of the electric vector position angle was found in optical and radio. The radio maps indicated a superluminal motion of 1.8±0.4c, which is the highest speed statistically significantly measured so far in a high-frequency-peaked BL Lac. For the first time, the high-energy bump in the broadband SED of 1ES 1011+496 could be fully characterized from 0.1 GeV to 1 TeV which permitted a more reliable interpretation within the one-zone SSC scenario. The polarimetry data suggest that at least part of the optical emission has its origin in some of the bright radio features, while the low polarization in optical might be due to the contribution of parts of the radio jet with different orientations of the magnetic field to the optical emission.